  Phase \RNum{2} of the LAMOST-{\sl Kepler/K}2 survey (LK-MRS), initiated in
2018, aims at collecting medium-resolution spectra ($R\sim7,500$; hereafter
MRS) for more than $50,000$ stars with multiple visits ($\sim60$ epochs) over a
period of 5 years (2018 September to 2023 June). We selected 20 footprints
distributed across the {\sl Kepler} field and six {\sl K}2 campaigns, with each
plate containing a number of stars ranging from $\sim2,000$ to $\sim 3,000$.
During the first year of observations, the LK-MRS has already collected
$\sim280,000$ and $\sim369,000$ high-quality spectra in the blue and red
wavelength range, respectively. The atmospheric parameters and radial
velocities for $\sim259,000$ spectra of $21,053$ targets were successfully
calculated by the LASP pipeline. The internal uncertainties for the effective
temperature, surface gravity, metallicity, and radial velocity are found to be
$100$\,K, $0.15$\,dex, $0.09$\,dex, and $1.00$\,km\,s$^{-1}$, respectively. We
found $14,997$, $20,091$, and $1,514$ stars in common with the targets from the
LAMOST low-resolution survey (LRS), GAIA and APOGEE, respectively,
corresponding to a fraction of $\sim70\%$, $\sim95\%$ and $\sim7.2\%$. In
general, the parameters derived from LK-MRS spectra are consistent with those
obtained from the LRS and APOGEE spectra, but the scatter increases as the
surface gravity decreases when comparing with the measurements from APOGEE. A
large discrepancy is found with the GAIA values of the effective temperature.
The comparisons of radial velocities of LK-MRS to GAIA and LK-MRS to APOGEE
nearly follow an Gaussian distribution with a mean $\mu\sim1.10$ and
$0.73$\,km\,s$^{-1}$, respectively.
