  In this paper, we have carried out a detailed study of the `Clocked' burster
GS $1826-238$ using $\sim$ 90 ks broad-band (0.7 - 60.0 keV) data obtained with
{\it AstroSat} observatory. The source was observed during a soft spectral
state and traced a `banana' type track in the colour-colour diagram (CCD). We
find that a combination of thermal component (multi-colour disc/bbodyrad) and
Comptonized component is statistically good description for all the sections of
the track in the CCD. The corona becomes optically thick ($\tau$ increases from
$\sim$ 5 to 21) and cooler ($kT_e$ decreases from $\sim$ 4.8 to 2.2 keV) as the
source moves up in the `banana' branch. Probably cooling is caused by increase
in the supply of soft-seed photons from the disc/boundary-layer. Reflection
signature is observed at upper `banana' branch of the source. Two type-I X-ray
bursts are detected during the {\it AstroSat} observations. During the bursts,
hard X-rays increased unlike previous observations where a reduction in hard
X-rays is observed during the bursts. Decrease in the electron temperature and
increase in the optical depth are observed during the bursts. The PSD (Power
Spectral Density) of all the sections of the CCD can be represented by a pure
power-law component. The strength of this component increases from $\sim$ 1\%
to 4.5\% as the source moves up in the `banana' track. Search for burst
oscillations gave a null result. We discuss the implications of our results in
the context of previous findings.
