  We propose a pebble-driven core accretion scenario to explain the formation
of giant planets around the late-M dwarfs of $M_{\star}{=}0.1{-}0.2 \
M_{\odot}$. In order to explore the optimal disk conditions for giant planet,
we perform N-body simulations to investigate the growth and dynamical evolution
of both single and multiple protoplanets in the disks with both inner viscously
heated and outer stellar irradiated regions. The initial masses of the
protoplanets are either assumed to be equal to $0.01 \ M_{\oplus}$ or
calculated based on the formula derived from streaming instability simulations.
Our findings indicate that massive planets are more likely to form in disks
with longer lifetimes, higher solid masses, moderate to high levels of disk
turbulence, and larger initial masses of protoplanets. In the single
protoplanet growth cases, the highest planet core mass that can be reached is
generally lower than the threshold necessary to trigger rapid gas accretion,
which impedes the formation of giant planets. Nonetheless, in multi-protoplanet
cases, the cores can exceed the pebble isolation mass barrier aided by frequent
planet-planet collisions. This consequently speeds up their gas accretion and
promotes giant planet formation, making the optimal parameter space to grow
giant planets substantially wider. Taken together, our results suggest that
even around very low-mass stellar hosts, the giant planets with orbital periods
of ${\lesssim}100$ days are still likely to form when lunar-mass protoplanets
first emerge from planetesimal accretion and then grow rapidly by a combination
of pebble accretion and planet-planet collisions in disks with a high supply of
pebble reservoir ${>}50 \ M_{\oplus}$ and turbulent level of $\alpha_{\rm t}
{\sim} 10^{-3}{-}10^{-2}$.
