  The recent theoretical advance known as the Minimal Geometric Deformation
(MGD) method has initiated a renewed interest in investigating higher curvature
gravitational effects in relativistic astrophysics. In this work, we model a
strange star within the context of Einstein-Gauss-Bonnet gravity with the help
of the MGD technique. Starting off with the Tolman metric ansatz together with
the MIT Bag model equation of state applicable to hadronic matter, anisotropy
is introduced via the superposition of the seed source and the decoupled
energy-momentum tensor. The solution of the governing systems of equations
bifurcates into two distinct models, namely the mimicking of the $\theta$
sector to the seed radial pressure and energy density and a regular fluid
model. Each of these models can be interpreted as self-gravitating static,
compact objects with the exterior described by the vacuum Boulware-Deser
solution. Utilizing observational data for three stellar candidates, viz., PSR
J1614-2230, PSR J1903+317, and LMC X-4 we subject our solutions to rigorous
viability tests based on regularity and stability. We find that the
Einstein-Gauss-Bonnet parameter and the decoupling constant compete against
each other for ensuring physically realizable stellar structures. The novel
feature of work is the demonstration of stable compact objects with stellar
masses in excess of $M= 2 M_{\odot}$ without appealing to exotic matter. The
analysis contributes new insights and physical consequences concerning the
development of ultra-compact astrophysical entities.
