  In this letter, we develop a model formalism to study the structure of a
relativistic, viscous, optically thin, advective accretion flow around a
rotating black hole in presence of radiative coolings. We use this model to
examine the physical parameters of the Ultra-luminous X-ray sources (ULXs),
namely mass ($M_{\rm BH}$), spin ($a_{\rm k}$) and accretion rate (${\dot m}$),
respectively. While doing this, we adopt a recently developed effective
potential to mimic the spacetime geometry around the rotating black holes. We
solve the governing equations to obtain the shock induced global accretion
solutions in terms of ${\dot m}$ and viscosity parameter ($\alpha$). Using
shock properties, we compute the Quasi-periodic Oscillation (QPO) frequency
($\nu_{\rm QPO}$) of the post-shock matter (equivalently post-shock corona,
hereafter PSC) pragmatically, when the shock front exhibits Quasi-periodic
variations. We also calculate the luminosity of the entire disc for these shock
solutions. Employing our results, we find that the present formalism is
potentially promising to account the observed $\nu_{\rm QPO}$ and bolometric
luminosity ($L_{\rm bol}$) of a well studied ULX source IC 342 X-1. Our
findings further imply that the central source of IC 342 X-1 seems to be
rapidly rotating and accretes matter at super-Eddington accretion rate provided
IC 342 X-1 harbors a massive stellar mass black hole ($M_{\rm BH} < 100
M_\odot$) as indicated by the previous studies.
