  We present the results from the spectral and timing analysis of the accreting
neutron star 1A~1744-361 from the \nustar{} observation performed in its 2022
outbursts. The unabsorbed bolometric X-ray luminosity during this observation
in the energy band $0.1-100\kev{}$ is $3.9\times 10^{37}$ erg~s$^{-1}$,
assuming a distance of $9$ kpc. During this observation, the source was in the
banana branch of the atoll track. The source spectrum exhibits relativistic
disc reflection and clear absorption features when an absorbed blackbody and
cut-off power-law model describes the continuum emission. The $3-50\kev{}$
source spectrum is well fitted using a model combination consisting of an
absorbed single-temperature blackbody and a reflection model along with the
addition of a warm absorber component. The inner-disk radius, $R_{in}$,
obtained from the reflection fit is $\sim(1.61-2.86)R_{ISCO}=(8.4-14.9)R_{g}$
($17.6-31.2$ km for a $1.4\Msun$ NS). This measurement allowed us to further
constrain the magnetic field strength to $B\lesssim 0.94\times 10^{9}$G. The
strong absorption features $\sim 6.91\kev{}$ and $\sim 7.99\kev{}$ imply the
presence of highly ionized absorbing material with a column density $N_{H}$ of
$\sim 3\times 10^{22}$ cm$^{-2}$, emanating from the accretion disk in the form
of disc wind with an outflow velocity of $v_{out}\simeq 0.021c\simeq 6300$ km
s$^{-1}$.
