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We report here CCD $I$-band time-series photometry of a young (2$-$5 Myr)cluster NGC 2282 to identify and understand the variability ofpre-main-sequence (PMS) stars. The $I$-band photometry, down to $\sim$ 20.5mag, enables us to probe the variability towards the lower mass end ($\sim$ 0.1M$_\odot$) of the PMS stars. From the light curves of 1627 stars, we identified62 new photometric variable candidates. Their association with the region wasestablished from H$\alpha$ emission and infrared (IR) excess. Among 62variables, 30 young variables exhibit H$\alpha$ emission, near-IR (NIR)/mid-IR(MIR) excess or both, and they are candidate members of the cluster. Out of 62variables, 41 are periodic variables with the rotation rate ranging from 0.2 to7 days. The period distribution exhibits a median period at $\sim$ 1-day as inmany young clusters (e.g., NGC~2264, ONC, etc.), but it follows a uni-modaldistribution unlike others having bimodality with the slow rotators peaking at$\sim$ 6$-$8 days. To investigate the rotation-disk and variability-diskconnection, we derived NIR excess from $\Delta$(I$-$K) and MIR excess from$Spitzer$ [3.6]$-$[4.5] $\mu$m data. No conclusive evidence of slow rotationwith the presence of disks around stars and fast rotation for diskless stars isobtained from our periodic variables. A clear increasing trend of thevariability amplitude with the IR excess is found for all variables.

Optical Photometric Variable Stars towards the Galactic \hii region NGC 2282