We report the statistical physical properties of the C$^{18}$O($J=1-0$) clumps present in a prominent cluster-forming region, Cygnus X, using the dataset obtained by the Nobeyama 45-m radio telescope. This survey covers 9 deg$^2$ of the north and south regions of Cygnus X, and totally 174 C$^{18}$O clumps are identified using the dendrogram method. Assuming a distance of 1.4 kpc, these clumps have radii of 0.2-1 pc, velocity dispersions of $<2.2~mathrm{km~s^{-1}}$, gas masses of 30-3000 $M_odot$, and H$_2$ densities of (0.2-5.5)$times10^4~mathrm{cm^{-3}}$. We confirm that the C$^{18}$O clumps in the north region have a higher H$_2$ density than those in the south region, supporting the existence of a difference in the evolution stages, consistent with the star formation activity of these regions. The difference in the clump properties of the star-forming and starless clumps is also confirmed by the radius, velocity dispersion, gas mass, and H$_2$ density. The average virial ratio of 0.3 supports that these clumps are gravitationally bound. The C$^{18}$O clump mass function shows two spectral index components, $alpha=-1.4$ in 55-140 $M_odot$ and $alpha=-2.1$ in $>140~M_odot$, which are consistent with the low- and intermediate-mass parts of the Kroupas initial mass function. The spectral index in the star-forming clumps in $>140~M_odot$ is consistent with that of the starless clumps in 55-140 $M_odot$, suggesting that the latter will evolve into star-forming clumps while retaining the gas accretion. Assuming a typical star formation efficiency of molecular clumps (10%), about ten C$^{18}$O clumps having a gas mass of $>10^3~M_odot$ will evolve into open clusters containing one or more OB stars.
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