  In order to understand the initial conditions and early evolution of star
formation in a wide range of Galactic environments, we carried out an
investigation of 64 \textit{Planck} Galactic Cold Clumps (PGCCs) in the second
quadrant of the Milky Way. Using the $^{13}$CO and C$^{18}$O $J = 1 - 0$ lines,
and 850\,$\mu$m continuum observations, we investigated cloud fragmentation and
evolution associated with star formation. We extracted 468 clumps and 117 cores
from the $^{13}$CO line and 850\,$\mu$m continuum maps, respectively. We make
use of the Bayesian Distance Calculator and derived the distances of all 64
PGCCs. We found that in general, the mass-size plane follows a relation of
$m\sim r^{1.67}$. At a given scale, the masses of our objects are around 1/10
of that of typical Galactic massive star-forming regions. Analysis of the clump
and core masses, virial parameters, densities, and mass-size relation suggests
that the PGCCs in our sample have a low core formation efficiency
($\sim$3.0\%), and most PGCCs are likely low-mass star-forming candidates.
Statistical study indicates that the 850\,$\mu$m cores are more turbulent, more
optically thick, and denser than the $^{13}$CO clumps for star formation
candidates, suggesting that the 850\,$\mu$m cores are likely more appropriate
future star-formation candidates than the $^{13}$CO clumps.
