The non-uniform distribution of gas and protostars in molecular clouds is caused by combinations of various physical processes that are difficult to separate. We explore this non-uniform distribution in the M17 molecular cloud complex that hosts massive star formation activity using the $^{12}$CO ($J=1-0$) and $^{13}$CO ($J=1-0$) emission lines obtained with the Nobeyama 45m telescope. Differences in clump properties such as mass, size, and gravitational boundedness reflect the different evolutionary stages of the M17-H{scriptsize II} and M17-IRDC clouds. Clumps in the M17-H{scriptsize II} cloud are denser, more compact, and more gravitationally bound than those in M17-IRDC. While M17-H{scriptsize II} hosts a large fraction of very dense gas (27%) that has column density larger than the threshold of $sim$ 1 g cm$^{-2}$ theoretically predicted for massive star formation, this very dense gas is deficient in M17-IRDC (0.46%). Our HCO$^+$ ($J=1-0$) and HCN ($J=1-0$) observations with the TRAO 14m telescope, { lqb trace all gas with column density higher than $3times 10^{22}$ cm$^{-2}$}, confirm the deficiency of high density ($gtrsim 10^5$ cm$^{-3}$) gas in M17-IRDC. Although M17-IRDC is massive enough to potentially form massive stars, its deficiency of very dense gas and gravitationally bound clumps can explain the current lack of massive star formation.
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