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The {\it Planck} Galactic Cold Clumps (PGCCs) are the possiblerepresentations of the initial conditions and the very early stages of starformation. With an objective to understand better the star and star clusterformation, we probe the molecular cloud associated with PGCC G108.37-01.06(hereafter, PG108.3), which can be traced in a velocity range $-$57 to $-$51 kms$^{-1}$. The IPHAS images reveal H$\alpha$ emission at various locationsaround PG108.3, and optical spectroscopy of the bright sources in those zonesof H$\alpha$ emission disclose two massive ionizing sources with spectral typeO8-O9V and B1V. Using the radio continuum, we estimate ionizing gas parametersand find the dynamical ages of \hii regions associated with the massive starsin the range 0.5$-$0.75 Myr. Based on the stellar surface density mapconstructed from the deep near-infrared CHFT observations, we find twoprominent star clusters in PG108.3; of which, the cluster associated with \hiiregion S148 is moderately massive ($\sim$ 240 M$\sun$). A careful inspection ofJCMT $^{13}$CO(3$-$2) molecular data exhibits that the massive cluster isassociated with a number of filamentary structures. Several embedded youngstellar objects (YSOs) are also identified in the PG108.3 along the length andjunction of filaments. We find the evidence of velocity gradient along thelength of the filaments. Along with kinematics of the filaments and thedistribution of ionized, molecular gas and YSOs, we suggest that the clusterformation is most likely due to the longitudinal collapse of the most massivefilament in PG108.3.

The Planck Cold Clump G108.37-01.06: A Site of Complex Interplay between H II Regions, Young Clusters and Filaments