  Galactic transient black hole candidate (BHC) MAXI J1535-571 was discovered
on 2017 September 02 simultaneously by {\it MAXI}/GSC and {\it Swift}/BAT
instruments. It has also been observed by India's first multi-wavelength
astronomy-mission satellite {\it AstroSat}, during the rising phase of its
2017-18 outburst. We make both the spectral and the temporal analysis of the
source during 2017 September 12-17 using data of {\it AstroSat}'s Large Area
X-ray Proportional Counter (LAXPC) in the energy range of $3-40$~keV to infer
the accretion flow properties of the source. Spectral analysis is done with the
physical two-component advective flow (TCAF) solution-based {\it fits} file.
From the nature of the variation of the TCAF model fitted physical flow
parameters, we conclude and confirm that the source was in the intermediate
spectral state during our analysis period. We observe sharp type-C
quasi-periodic oscillations (QPOs) in the frequency range of $\sim
1.75-2.81$~Hz. For a better understanding of the nature and evolution of these
type-C QPOs, a dynamic study of the power density spectra is done. We also
investigate the origin of these QPOs from the shock oscillation model. We find
that non-satisfaction of Rankine-Hugoniot conditions for non-dissipative shocks
and not their resonance oscillations is the cause of the observed type-C QPOs.
