  We use a set of hadronic equations of state derived from covariant density
functional theory to study the impact of their high-density behavior on the
properties of rapidly rotating $\Delta$-resonance-admixed hyperonic compact
stars. In particular, we explore systematically the effects of variations of
the bulk energy isoscalar skewness, $Q_{\mathrm{sat}}$, and the symmetry energy
slope, $L_{\mathrm{sym}}$, on the masses of rapidly rotating compact stars.
With models for equation of state satisfying all the modern astrophysical
constraints, excessively large gravitational masses of around $2.5 \,
M_{\odot}$ are only obtained under three conditions: (a) strongly attractive
$\Delta$-resonance potential in nuclear matter, (b) maximally fast (Keplerian)
rotation, and (c) parameter ranges $Q_{\mathrm{sat}}\gtrsim500$ MeV and
$L_{\mathrm{sym}}\lesssim50$ MeV. These values of $Q_{\mathrm{sat}}$ and
$L_{\mathrm{sym}}$ have a rather small overlap with a large sample (total of
about 260) parametrizations of covariant nucleonic density functionals. The
extreme nature of requirements (a)-(c) reinforces the theoretical expectation
that the secondary object involved in the GW190814 event is likely to be a
low-mass black hole rather than a supramassive neutron star.
