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This paper presents photometric, astrometric, and kinematic analyses of theopen clusters NGC 189, NGC 1758 and NGC 7762 based on CCD UBV photometric andGaia Data Release 3 (DR3) data. According to membership analyses, we identified32, 57 and 106 most probable member stars with membership probabilities $P\geq0.5$ in NGC 189, NGC 1758 and NGC 7762, respectively. The color excesses andphotometric metallicities of each cluster were determined separately using UBVtwo-color diagrams. The color excess $E(B-V)$ is $0.590 \pm 0.023$ mag for NGC189, $0.310 \pm 0.022$ mag for NGC 1758 and $0.640 \pm 0.017$ mag for NGC 7762.The photometric metallicity [Fe/H] is $-0.08 \pm 0.03$ dex for both NGC 189 andNGC 1758, and $-0.12 \pm 0.02$ dex for NGC 7762. Distance moduli and ages ofthe clusters were obtained by comparing PARSEC isochrones with thecolor-magnitude diagrams constructed from UBV and Gaia photometric data. Duringthis process, we kept as constant color excess and metallicity for eachcluster. The estimated isochrone distance is $1201 \pm 53$ pc for NGC 189, $902\pm 33$ pc for NGC 1758 and $911 \pm 31$ pc for NGC 7762. These are compatiblewith the values obtained from trigonometric parallax. Ages of the clusters are$500\pm 50$ Myr, $650\pm 50$ Myr and $2000\pm 200$ Myr for NGC 189, NGC 1758and NGC 7762, respectively. Galactic orbit integration of the clusters showedthat NGC 1758 completely orbits outside the solar circle, while NGC 189 and NGC7762 enter the solar circle during their orbits.

CCD UBV and Gaia DR3 based analysis of NGC 189, NGC 1758 and NGC 7762 open clusters