  When rotating primordial black holes evaporate via Hawking radiation, their
rotational energy and mass are dissipated with different dynamics. We
investigate the effect of these dynamics on the production of dark radiation --
in the form of hot gravitons or vector bosons -- and non-cold dark matter.
Although the production of higher-spin particles is enhanced while primordial
black holes are rotating, we show that the energy density of dark radiation
experiences an extra redshift because their emission effectively halts before
PBH evaporation completes. We find that taking this effect into account leads
to suppression by a factor of $\mathcal{O}(10)$ of $\Delta N_{\rm eff}$ for
maximally rotating black holes as compared to previous results. Using the
solution of the Friedmann and Boltzmann equations to accurately calculate the
evolution of linear perturbations, we revisit the warm dark matter constraints
for light candidates produced by evaporation and how these limits vary over
black hole spins. Due to the interplay of enhanced production and late
dilution, we obtain that higher spin particles are most affected by these
bounds. Our code FRISBHEE, FRIedmann Solver for Black Hole Evaporation in the
Early universe, developed for this work can be found at
https://github.com/yfperezg/frisbhee
