  The properties of rotating neutron stars are investigated using eight
equations of state (EOSs). We also study the relations between various
observables corresponding to different angular velocities for all those EOSs.
All of these EoSs lead to non-rotating compact stars with maximum masses
between 1.8 to 2.25 $M_{\odot}$. We calculate the moment of inertia and studied
its variation with mass and the relation between central energy density and
angular momentum. We compare our results with the observational findings from
the most massive pulsar PSR J0740+6620 and the heaviest secondary component in
the black hole - neutron star merger GW190814. It is noted that the secondary
compact object of GW190814 having mass $\sim 2.6 M_{\odot}$ might be explained
as a rapidly rotating neutron star (NS) with frequency larger than 1000 Hz.
