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The star formation history (SFH) and the properties of the dwarf galaxy LGS3are analyzed using color-magnitude (CM) diagrams plotted from VRI photometry of736 stars. The distance to the galaxy is estimated through the position of thetip or the red giant branch. Two acceptable results have been obtained:0.77+/-0.07 Mpc and 0.96+/-0.07 Mpc, although the first value is favored bycomplementary considerations on the stellar content of the galaxy. Both valuesmake LGS3 a possible satellite of M31 or of M33. The SFH is investigated foreach of the two adopted distances comparing the observed CM diagrams with modelCM diagrams computed for different star formation rates (psi(t)) and chemicalenrichment laws (Z(t)).  The results are compatible with LGS3 having been forming stars since an earlyepoch, 15-12 Gyr ago, at an almost constant rate if distance is 0.77 Mpc or atan exponentially decreasing rate if distance is 0.96 Mpc. According to ourmodels, the current metallicity would range from Z~0.0007 to Z~0.002. Otherresults are the current psi(t): (0.55+/-0.04)x10^(-10) Mo yr^(-1) pc^(-2) or(0.47+/-0.07)x10^(-10) Mo yr^(-1) pc^(-2), depending of the distance, and itsaverage for the entire life of the galaxy, <psi>=(1.4+/-0.1)x10^(-10) Moyr^(-1) pc^(-2). At the present psi(t), the probability of LGS3 having an HIIregion is 0.2, which is compatible with the fact that no HII regions have beenfound in the galaxy. Its fraction of gas relative to the mass intervening inthe chemical evolution is about 0.40 and its percentage of dark matter (thatwhich cannot be explained as stellar remnants or by extrapolation of the usedIMF to low masses) is 95%. The results for psi(t) and Z(t) for d=0.77 Mpc arecompatible with a moderate outflow of well mixed material (lambda=3), but largeComment: 23 pages, 3 tables, 14 figures. AJ in pres

The Stellar Content and the Star Formation History of the Local Group Dwarf Galaxy LGS 3.