This paper presents photometric, astrometric, and kinematic analyses of the open clusters NGC 189, NGC 1758 and NGC 7762 based on CCD UBV photometric and Gaia Data Release 3 (DR3) data. According to membership analyses, we identified 32, 57 and 106 most probable member stars with membership probabilities P⩾0.5 in NGC 189, NGC 1758 and NGC 7762, respectively. The color excesses and photometric metallicities of each cluster were determined separately using UBV two-color diagrams. The color excess E(B-V) is 0.590±0.023 mag for NGC 189, 0.310±0.022 mag for NGC 1758 and 0.640±0.017 mag for NGC 7762. The photometric metallicity [Fe/H] is -0.08±0.03 dex for both NGC 189 and NGC 1758, and -0.12±0.02 dex for NGC 7762. Distance moduli and ages of the clusters were obtained by comparing PARSEC isochrones with the color-magnitude diagrams constructed from UBV and Gaia photometric data. During this process, we kept as constant color excess and metallicity for each cluster. The estimated isochrone distance is 1201±53 pc for NGC 189, 902±33 pc for NGC 1758 and 911±31 pc for NGC 7762. These are compatible with the values obtained from trigonometric parallax. Ages of the clusters are 500±50 Myr, 650±50 Myr and 2000±200 Myr for NGC 189, NGC 1758 and NGC 7762, respectively. Galactic orbit integration of the clusters showed that NGC 1758 completely orbits outside the solar circle, while NGC 189 and NGC 7762 enter the solar circle during their orbits.