The membership determination for open clusters in noisy environments of the Milky Way is still an open problem. In this paper, our main aim is provide the membership probability of stars using proper motions and parallax values of stars using Gaia EDR3 astrometry. Apart from the Gaia astrometry, we have also used other photometric data sets like UKIDSS, WISE, APASS and Pan-STARRS1 in order to understand cluster properties from optical to mid-infrared regions. We selected 438 likely members with membership probability higher than $50%$ and G$le$20 mag. We obtained the mean value of proper motion as $mu_{x}=1.27pm0.001$ and $mu_{y}=-0.73pm0.002$ mas yr$^{-1}$. The clusters radius is determined as 7.5 arcmin (5.67 pc) using radial density profile. Our analysis suggests that NGC 1348 is located at a distance of $2.6pm0.05$ kpc. The mass function slope is found to be $1.30pm0.18$ in the mass range 1.0$-$4.1 $M_odot$, which is in fair agreement with Salpeters value within the 1$sigma$ uncertainty. The present study validates that NGC 1348 is a dynamically relaxed cluster. We computed the apex coordinates $(A, D)$ for NGC 1348 as $(A_circ, D_circ)$ = $(-23^{textrm{o}}.815pm 0^{textrm{o}}.135$, $-22^{textrm{o}}.228pm 0^{textrm{o}}.105)$. In addition, calculations of the velocity ellipsoid parameters (VEPs), matrix elements $mu_{ij}$, direction cosines ($l_j$, $m_j$, $n_j$) and the Galactic longitude of the vertex have been also conducted in this analysis.
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