  We present the detection of type C quasi-periodic oscillation (QPO) along
with upper harmonic at respective frequencies of $\sim0.6$ Hz and $\sim1.2$ Hz
in the single AstroSat observation taken during the 2016 outburst of the
low-mass black hole X-ray binary H~1743--322. These frequencies are found to be
shifted by $\sim0.4$ Hz for the QPO and $\sim0.8$ Hz for the upper harmonic
with respect to that found in the simultaneous \textit{XMM-Newton} and
\textit{NuSTAR} observation taken five days later than the AstroSat
observation, indicating a certain geometrical change in the system. However,
the centroid frequency of the QPO and the upper harmonic do not change with
energy, indicating the energy-independent nature. The decreasing trend in the
fractional rms of the QPO with energy is consistent with the previous results
for this source in the low/hard state. The value of the photon index
($\Gamma\sim1.67$) also indicates that the source was in the low/hard state
during this particular observation. In addition, similar to the
\textit{XMM-Newton} observations during the same outburst, we find a hard lag
of $\sim21$ ms in the frequency range of $\sim1-5$ Hz. The log-linear trend
between the averaged time lag and energy indicates the propagation of
fluctuations in the mass accretion rate from outer part of the accretion disk
to the inner hot regions.
