  Inspired by the conundrum of the gravitational event, GW190814 which brings
to light the coalescence of a 23 $ M_{\odot}$ black hole with a yet to be
determined secondary component, we look to modelling compact objects within the
framework of $f(\mathcal{Q})$ gravity by employing the method of gravitational
decoupling. We impose a quadratic equation of state (EOS) for the interior
matter distribution which in the appropriate limit reduces to the MIT bag
model. The governing field equations arising from gravitational decoupling
bifurcates into the $\rho=\theta^0_0$ and $p_r=\theta^1_1$ sectors leading to
two distinct classes of solutions. Both families of solutions are subjected to
rigorous tests qualifying them to describe a plethora of compact objects
including neutron stars, strange stars and the possible progenitor of the
secondary component of GW190814. Using observational data of mass-radius
relations for compact objects LMC X-4, Cen X-3, PSR J1614-2230 and PSR
J0740+6620 we show that it is possible to generate stellar masses and radii
beyond 2.0 $ M_{\odot}$ for neutron stars. Our findings reveal that the most {
suitable and versatile model in this framework is the quadratic EOS}, which
accounts for a range of low mass stars as well as typical stellar candidates
describing the secondary component of GW190814.
