  We present an analysis of high latitude $\delta$ Scuti stars
($\left|b\right|> 1^{\circ}$) in the Galactic bulge region ($-8^{\circ}.3<
l<9^{\circ}.4$) using a clean sample of the photometric data of $7,440$ stars
recently released by the OGLE-IV project. The geometrical parameters of the
bulge are determined based on Maximum Likelihood (ML) analysis in
five-dimensional parameter space. More refined values of these parameters as
well as their uncertainties are obtained from a fully Bayesian Markov Chain
Monte Carlo (MCMC) analysis. Approximating the bulge as an ellipsoid, the
distribution of the number density of stars as a function of Galacto-centric
distance has been modelled using three distribution functions: two Exponential
($\rm E_{1},\rm E_{2}$) types and one Gaussian ($\rm G$) type. Based on the AIC
and BIC values, the exponential model $\rm E_{1}$ is chosen as the best
statistical model for the parameter values obtained from the MCMC analysis. The
MCMC analysis yields the following results: the mean distance to the Galactic
center (GC) is found to be $R_{0}=8.034\pm0.012_{\rm stat}\pm0.586_{\rm sys}$
kpc; the bulge $\delta$ Scuti distribution has a triaxial shape with normalized
($a\equiv1$) axes ratios ($a:b:c$) as $1.000\pm
0.005:0.348\pm0.002:0.421\pm0.002$. Here $a$ is the semi-major axis lying in
the Galactic plane and pointing towards us; $b$ and $c$ are the two semi-minor
axes, the former lying in the Galactic plane and the later perpendicular to it.
Smaller values of $b$ as compared to $a$ obtained for Galacto-centric distances
$R\ge 2.0$~kpc indicate the presence of a bar-like structure of the bulge with
a bar angle of $22^{\circ}.006\pm2^{\circ}.078$.
