16 may form a larger group with 19, 21 and 22. Their ages are consistent with 16 this hypothesis. 19 may form a larger group with 16, 21 and 22. Their ages are consistent with 19 this hypothesis. 21 may form a larger group with 16, 19 and 22. Their ages are consistent with 21 this hypothesis. 22 may form a larger group with 16, 19 and 21. Their ages are consistent with 22 this hypothesis. 27 and 28: Their brightest members are close to a bright foreground star, 27 which may alter their photometry. The affected members are discarded. 28 and 27: Their brightest members are close to a bright foreground star, 28 which may alter their photometry. The affected members are discarded. 34 The two brightest members (id: 32277, 32501) are blended and therefore 34 discarded for age and mass determination. 48 Visual inspection reveals a blue gaseous filament overlapping with 48 association members. Spitzer observations at 8um, which traces PAH and hot 48 dust, found a peak in the area covered by associations 43, 44 and 48. 57 57's brightest member may be contaminated by a nearby object. 66 Visual inspection revealed that the brightest member, with very red B-V, 66 is an extended source. This target was discarded. 72 72's brightest member may be contaminated by a nearby object. 76 and 77 are 72 only 7" away. Their populations exhibit a similar age distribution. 82 The two brightest members are very close to each other but well resolved 82 in WFPC2 images. 86 Its brightest member shows a lobular shape in WFPC2 images, suggesting that 86 it may be an unresolved triple system. 88 Its B-V vs. V diagram is bimodal, one set of stars following the main 88 sequence and the other having redder B-V colors. The stars in the latter 88 sequence look extended in the INT images, hence were discarded for age 88 and mass determination. 104 Its brightest member (id: 52443) may be contaminated by a nearby object. 107 This association was discarded because it only has two valid members. It is 107 close to 106; the age of the remaining members is in agreement with 107 that of 106. 112 The two brightest members are very close to each other, and might be not 112 well resolved by our photometric reduction. 113 Extra-reddening is seen in the B-V vs. V diagram as an offset. 114 The three brightest blue members are very close to each other, but well 114 resolved in VLT-VIMOS images. After cleaning the Q vs. Vcorr diagram from 114 a vertical sequence of stars with redder Q which seem to be blends in the 114 images, there is a very well defined sequence of stars following 114 the 7.1 isochrone. 120 The brightest members are very close to each other. 125 Its brightest member could be contaminated by a nearby red star, although 125 its normal colors suggest otherwise. 134 All members have Q color bluer than the youngest isochrone. The brightest 134 member, however, is close to the 5.9 isochrone within the analysis errors, 134 and was used for age and mass determination. 135 See Sect. 2.3. 151 is the most populated association of our catalog. It includes IC 1613's 151 supernova remnant (SNR). Our catalog's entries for the SNR are discarded 151 for age and mass determination. 153 153's brightest star was discarded because it is blended with a nearby 153 object. 154 encloses IC 1613's known oxygen Wolf-Rayet, found by Dodorico & Rosa 154 (1982A&A...105..410D). Some entries of our OB-star candidate list are knots 154 of the nebula ionized by the WR and discarded for age and mass 154 determination. The points left do not allow us to derive the association \ 154 age; the value listed in Table 1 is the age of evolutionary points of 154 Z=0.004 with surface abundances matching those derived for the WO by 154 Kingsburgh & Barlow (1995A&A...295..171K), and similar Teff and Lbol. 154 Those points correspond to an initial mass ranging from 60M_{sun}_ to 154 120M_{sun}_, having currently ~10M_{sun}_. Since the present analysis does 154 not allow us to refine the result any further, these values were not 154 provided in columns MupI-MupC. 157 The brightest star is triple in VLT-VIMOS images but unresolved in our 157 catalog. 158 contains 64 029 (or V39 ([S71b] V39 in simbad)), the Luminous Blue 158 Variable candidate (LBVc) we report in Herrero et al. 158 (2010A&A...513A..70H). 160 160's brightest star (id: 64338) could be blended to another member 160 (id: 64346). 185 The association displays a very high stellar density. The brightest members 185 might be contaminated by nearby objects. 192 There may be contamination of the brightest star with a red star. The pair 192 is resolved in VLT-VIMOS R-band images. All members have Q color bluer than 192 the youngest isochrone, hence the association is classified "dubious" and 192 we provide NOB=0 in Table 1. We adopted logAge=5.9. 194 The brightest object of this association is discarded, because it is an 194 edge-on background spiral galaxy. 195 The brightest object of this association is discarded, because it likely is 195 a background galaxy. 197 The brightest member (id: 75661) is discarded for age and mass determination 197 because of its very blue Q color and because it may be contaminated by a 197 nearby object.