  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 $P\geq
0.5$ 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 $0.590 \pm 0.023$ mag for NGC
189, $0.310 \pm 0.022$ 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 and
NGC 1758, and $-0.12 \pm 0.02$ 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 $1201 \pm 53$ pc for NGC 189, $902
\pm 33$ pc for NGC 1758 and $911 \pm 31$ pc for NGC 7762. These are compatible
with 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 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.
