  We present photometric and kinematic analysis of an intermediate age open
cluster NGC 1027 using $UBV(RI)_c$ and Gaia Early Data Release 3 (EDR3) data.
Structural and fundamental parameters such as cluster center, cluster extent,
reddening, age and distance are estimated in this study. Cluster center is
found about 2 arcmin away from the center reported earlier. Radius has been
estimated to be about 8.00 arcmin(2.65pc). Using proper motion Gaia EDR3 data,
membership probabilities has been derived for the stars in the region of
cluster radius. We find mean proper motion of the cluster to be $\sim$(-0.84,
2.04) mas yr$^{-1}$ in (RA, DEC). We find 217 most probable (P$_\mu>$ 70\%)
cluster members with mean parallax 0.892 $\pm$ 0.088 mas. Out of these, 160
members have counterparts in our optical observations. Few stars having
P$_\mu>$ 70\% are found out of the cluster radius showing imprints of dynamical
evolution. The color-color and color-magnitude diagrams for the cluster members
found within 8.00 arcmin have been constructed using $UBV(RI)_c$ photometry and
Gaia EDR3 data. This yields a reddening E($B$-$V$) $\sim$ 0.36 mag, age $\sim$
130 Myr and distance $\sim$ 1.14 kpc. The mass function slope in the cluster
region is $\Gamma$ $\sim$ -1.46 $\pm$ 0.15, which is similar to other Galactic
open clusters. The dynamical study shows lack of faint stars in its inner
region leading to mass segregation effect. A comparison of dynamical age with
cluster age indicates that NGC 1027 is a dynamically relaxed cluster suggesting
that mass segregation may be imprint of its dynamical relaxation.
