  How diffuse dwarf galaxies that are deficient in dark matter -- such as
NGC1052-DF2 and NGC1052-DF4 -- formed remains a mystery. Along with their
luminous member globular clusters (GCs), the so-called dark matter deficient
galaxies (DMDGs) have challenged observers and theorists alike. Here we report
a suite of galaxy collision simulations using the adaptive mesh refinement code
ENZO with 1.25 pc resolution, which demonstrates that high-velocity galaxy
collisions induce the formation of DMDGs and their star clusters (SCs)
simultaneously. With a numerical resolution significantly better than our
previous study (Shin et al. 2020), we resolve the dynamical structure of the
produced DMDGs and the detailed formation history of their SCs which are
possible progenitors of the DMDG's member GCs. In particular, we show that a
galaxy collision with a high relative velocity of $\sim 300\;{\rm km\;s}^{-1}$,
invoking severe shock compression, spawns multiple massive SCs ($\gtrsim
10^{6}\;{\rm M}_{\odot}$) within 150 Myr after the collision. At the end of our
~ 800 Myr fiducial run, the resulting DMDG of $M_{\star} \simeq 3.5\times
10^{8}\;{M}_{\odot}$ hosts 10 luminous ($M_{\rm V} \lesssim -8.5\;{\rm mag}$),
gravitational bound SCs with a line-of-sight velocity dispersion $11.2\;{\rm
km\;s}^{-1}$. Our study suggests that DMDGs and their luminous member SCs could
form simultaneously in high-velocity galaxy collisions while being in line with
the key observed properties of NGC1052-DF2 and NGC1052-DF4.
