  We show that the odds of the mass-gap (secondary) object in GW190814 being a
neutron star (NS) improve if one allows for a stiff high-density equation of
state (EoS) or a large spin. Since its mass is $\in (2.50,2.67) M_{\odot}$,
establishing its true nature will make it either the heaviest NS or the
lightest black hole (BH), and can have far-reaching implications on NS EoS and
compact object formation channels. When limiting oneself to the NS hypothesis,
we deduce the secondary's properties by using a Bayesian framework with a
hybrid EoS formulation that employs a parabolic expansion-based nuclear
empirical parameterization around the nuclear saturation density augmented by a
generic 3-segment piecewise polytrope (PP) model at higher densities and
combining a variety of astrophysical observations. For the slow-rotation
scenario, GW190814 implies a very stiff EoS and a stringent constraint on the
EoS specially in the high-density region. On the other hand assuming the
secondary object is a rapidly rotating NS, we constrain its rotational
frequency to be $f=1170^{+389}_{-495}$ Hz, within a $90\%$ confidence interval.
In this scenario, the secondary object in GW190814 would qualify as the fastest
rotating NS ever observed. However, for this scenario to be viable, rotational
instabilities would have to be suppressed both during formation and the
subsequent evolution until merger, otherwise the secondary of GW190814 is more
likely to be a BH.
