  The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Low
Resolution Spectroscopic Survey (LRS) provides massive spectroscopic data of
M-type stars, and the derived stellar parameters could bring vital help to
various studies. We adopt the ULySS package to perform $\chi^2$ minimization
with model spectra generated from the MILES interpolator, and determine the
stellar atmospheric parameters for the M-type stars from LAMOST LRS Data
Release (DR) 8. Comparison with the stellar parameters from APOGEE Stellar
Parameter and Chemical Abundance Pipeline (ASPCAP) suggests that most of our
results have good consistency. For M dwarfs, we achieve dispersions better than
74 K, 0.19 dex and 0.16 dex for $T_{\rm eff}$, $\log{g}$ and [Fe/H], while for
M giants, the internal uncertainties are 58 K, 0.32 dex and 0.26 dex,
respectively. Compared to ASPCAP we also find a systematic underestimation of
$\Delta {T_{\rm eff}} =$ $-$176 K for M dwarfs, and a systematic overestimation
of $\Delta {\log{g}} =$ 0.30 dex for M giants. However, such differences are
less significant when we make comparison with common stars from other
literature, which indicates that systematic biases exist in the difference of
ASPCAP and other measurements. A catalog of 763,136 spectra corresponding to
616,314 M-type stars with derived stellar parameters is presented. We determine
the stellar parameters for stars with $T_{\rm eff}$ higher than 2,900 K, with
$\log{g}$ from -0.24 dex to 5.9 dex. The typical precisions are 45 K, 0.25 dex
and 0.22 dex, for $T_{\rm eff}$, $\log{g}$ and [Fe/H], respectively, which are
estimated from the duplicate observations of the same stars.
