  Recent numerical simulations have shown that the unstable disk within the
central regime of the primordial gas cloud fragments to form multiple
protostars on several scales. Their evolution depends on the mass accretion
phenomenon, interaction with the surrounding medium and radiative feedback
respectively. In this work, we use a fast semi-analytical framework in order to
model multiple protostars within a rotating cloud, where the mass accretion is
estimated via a Bondi-Hoyle flow and the feedback process is approximated
through radiation pressure. We observe that while some of the evolving
protostars possibly grow massive ($\approx 1-24 M_{\odot}$) via accretion and
mergers, a fraction of them ($\approx 20\%$) are likely to be ejected from the
parent cloud with a mass corresponding to $M_{*} \lesssim 0.8 M_{\odot}$. These
low-mass protostars may be considered as the potential candidates to enter the
zero-age-main-sequence (ZAMS) phase and possibly survive till the present
epoch.
