  Ultra-low mass primordial black holes (PBH), which may briefly dominate the
energy density of the universe but completely evaporate before the big bang
nucleosynthesis (BBN), can lead to interesting observable signatures. In our
previous work, we studied the generation of a doubly peaked spectrum of induced
stochastic gravitational wave background (ISGWB) for such a scenario and
explored the possibility of probing a class of baryogenesis models wherein the
emission of massive unstable particles from the PBH evaporation and their
subsequent decay contributes to the matter-antimatter asymmetry. In this work,
we extend the scope of our earlier work by including spinning PBHs and consider
the emission of light relativistic dark sector particles, which contribute to
the dark radiation (DR) and massive stable dark sector particles, thereby
accounting for the dark matter (DM) component of the universe. The ISGWB can
probe the non-thermal production of these heavy DM particles, which cannot be
accessible in laboratory searches. For the case of DR, we find a novel
complementarity between the measurements of $\Delta N_{\rm eff}$ from these
emitted particles and the ISGWB from PBH domination. Our results indicate that
the ISGWB has a weak dependence on the initial PBH spin. However, for gravitons
as the DR particles, the initial PBH spin plays a significant role, and only
above a critical value of the initial spin parameter $a_*$, which depends only
on initial PBH mass, the graviton emission can be probed in the CMB-HD
experiment. Upcoming CMB experiments such as CMB-HD and CMB-Bharat, together
with future GW detectors like LISA and ET, open up an exciting possibility of
constraining the PBHs parameter space providing deeper insights into the
expansion history of the universe between the end of inflation and BBN.
