  In the frame of Gauss-Bonnet gravity and in the limit of $D\to 4$, based on
the fact that spherically symmetric solution derived using any of
regularization schemes will be the same form as the original theory
\cite{Banerjee:2020yhu,Hennigar:2020lsl,Casalino:2020kbt,Aoki:2020lig}, we
derive a new interior spherically symmetric solution assuming specific forms of
the metric potentials that have two constants . Using the junction condition we
determine these two constants. By using the data of the star EXO $1785-248 $,
whose mass is $ { M=1.3\pm0.2 \,{\textrm M}_\odot}$ and radius $ {
l=8.849\pm0.4\,{\textrm km}}$, we calculate the numerical values of these
constants, in terms of the dimensionful coupling parameter of the Gauss-Bonnet
term, and eventually, we get real values for these constants. In this regard,
we show that the components of the energy-momentum tensor has a finite value at
the center of the star as well as a smaller value to the surface of the star.
Moreover, we show that the equations of the state behave in a non-linear way
due to the impact of the Gauss-Bonnet term. Using the
Tolman-Oppenheimer-Volkoff equation, the adiabatic index, and stability in the
static state we show that the model under consideration is always stable.
Finally, the solution of this study is matched with observational data of other
pulsars showing satisfactory results
