  We present the results obtained from detailed timing and spectral studies of
a black hole candidate MAXI~J1813-095 using {\it Swift}, {\it NICER}, and {\it
NuSTAR} observations during its 2018 outburst. The timing behaviour of the
source is mainly studied by using {\it NICER} light curves in a $0.5-10$ keV
range. We did not find any signature of quasi-periodic oscillations in the
power density spectra of the source. We carry out spectral analysis with a
combined disk blackbody \& power-law model, and a physical two-component
advective flow (TCAF) model. From the combined {\tt disk blackbody} \& {\tt
power-law} model, we extracted thermal and non-thermal fluxes, photon index,
and inner disk temperature. We also find evidence for weak reflection in the
spectra. We have tested the physical TCAF model on a broadband spectrum from
{\it NuSTAR} and {\it Swift}/XRT. The parameters like mass accretion rates, the
size of the Compton clouds and the shock strength are extracted. Our result
shows that the source remained in the hard state during the entire outburst
which indicates a `failed' outburst. We estimate the mass of the black hole as
$7.4 \pm 1.5$ $M_{\odot}$ from the spectral study with the TCAF model. We use
{\tt LAOR} model for the Fe K$\alpha$ line emission. From this, the spin
parameter of the black hole is estimated as $a^* > 0.76$. The inclination angle
of the system is estimated to be in the range of $28^{\circ} - 45^{\circ}$ from
the reflection model. We estimate the source distance to be $\sim 6$ kpc.
