  This study simulates strange stars in $f(Q)$ gravity with an additional
source under an electric field using gravitational decoupling and the complete
Gravitational Decoupling (CGD) technique. By employing the Tolman ansatz and
the MIT bag model equation of state (EOS), we explore bounded star
configurations derived from the $\theta_0^0 = \rho$ and $\theta_1^1 = p_r$
sectors within the CGD formalism. Our models are subjected to physical
viability tests, and we analyze the impact of anisotropy and the electric
charge parameter $E_0$ as well as the coupling parameters $\alpha$ and
$\beta_1$. Comparisons are made with observational constraints, including
GW190814, neutron stars PSR J1614-2230, PSR J1903+6620, Cen X-3 and LMC X-4.
Notably, we achieve the presence of a lower "\textit{mass gap}" component by
adjusting parameters $\alpha$ and $\beta_1$. Our models exhibit well-behaved
mass profiles, internal regularity, and stability, with the absence of
gravitational collapse verified through the Buchdahl--Andr\'{e}asson's limit.
In addition, we present a detailed physical analysis based on three parameters,
$\alpha$ (decoupling strength), $\beta_1$ ($f(Q)$--coupling) and $Q$ (surface
charge). This study provides insights into the behavior of compact objects in
$f(Q)$ gravity and expands our understanding of strange star configurations
within this framework.
