  We present an in-depth spectral and timing analysis of the Black Hole binary
4U 1630-472 during 2016 and 2018 outbursts as observed by \textit{AstroSat} and
\textit{MAXI}. The extensive coverage of the outbursts with \textit{MAXI} is
used to obtain the Hardness Intensity Diagram (HID). The source follows a
`c'-shaped profile in agreement with earlier findings. Based on the HIDs of
previous outbursts, we attempt to track the evolution of the source during a
`super'-outburst and `mini'-outbursts. We model the broadband energy spectra
($0.7-20.0$ keV) of \textit{AstroSat} observations of both outbursts using
phenomenological and physical models. No Keplerian disc signature is observed
at the beginning of 2016 outburst. However, the disc appears within a few hours
after which it remains prominent with temperature ($T_{in}$) $\sim$ 1.3 keV and
increase in photon index ($\Gamma$) from 1.8 to 2.0, whereas the source was at
a disc dominant state throughout the \textit{AstroSat} campaign of 2018
outburst. Based on the HIDs and spectral properties, we classify the outbursts
into three different states - the `canonical' hard and soft states along with
an intermediate state. Evolution of rms along different states is seen although
no Quasi-periodic Oscillations (QPOs) are detected. We fit the observed spectra
using a dynamical accretion model and estimate the accretion parameters. Mass
of the black hole is estimated using inner disc radius, bolometric luminosity
and two component flow model to be $3-9$ $M_{\odot}$. Finally, we discuss the
possible implications of our findings.
