  We present a statistical and multiwavelength photometric studies of young
open cluster IC 1590. We identified 91 cluster members using $Gaia$ DR3
astrometry data using ensemble-based unsupervised machine learning techniques.
From $Gaia$ EDR3 data, we estimate the best-fitted parameters for IC 1590 using
the Automated Stellar Cluster Analysis package (ASteCA) yielding the distance
$d$ $\sim$ 2.87 $\pm$ 0.02 Kpc, age $\sim$ 3.54 $\pm$ 0.05 Myr, metallicity $z$
$\sim$ 0.0212 $\pm$ 0.003, binarity value of $\sim$ 0.558, and extinction $A_v$
$\sim$ 1.252 $\pm$ 0.4 mag for an $R_v$ value of $\sim$ 3.322 $\pm$ 0.23. We
estimate the initial mass function slope of the cluster to be $\alpha$ = 1.081
$\pm$ 0.112 for single stars and $\alpha$ = 1.490 $\pm$ 0.051 for a binary
fraction of $\sim$ 0.558 in the mass range 1 M$_{\odot}$ $\leq$ m(M$_{\odot}$)
$\leq$ 100 M$_{\odot}$. The $G$-band luminosity function slope is estimated to
be $\sim$ 0.33 $\pm$ 0.09. We use $(J-H)$ versus $(H-K_s)$ color-color diagram
to identify young stellar objects (YSOs). We found that all the identified YSOs
have ages $\leq$ 2 Myr and masses $\sim$ 0.35 - 5.5 M$_{\odot}$. We also fit
the radial surface density profile. Using the galpy we performed orbit analysis
of the cluster. The extinction map for the cluster region has been generated
using the PNICER technique and it is almost similar to the dust structure
obtained from the 500 $\mu$$m$ dust continuum emissions map of $Herschel$
SPIRE. We finally at the end discussed the star formation scenario in the
cluster region.
