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We present $^{12}$CO ($J$ = 2-1), $^{13}$CO ($J$ = 2-1), and C$^{18}$O ($J$ =2-1) observations toward GMC-8, one of the most massive giant molecular clouds(GMCs) in M33 using ALMA with an angular resolution of 0".44 $\times$ 0".27($\sim$2 pc $\times$ 1pc). The earlier studies revealed that its high-mass starformation is inactive in spite of a sufficient molecular reservoir with thetotal mass of $\sim$10$^{6}$ $M_{\odot}$.  The high-angular resolution data enable us to resolve this peculiar sourcedown to a molecular clump scale. One of the GMC's remarkable features is that around-shaped gas structure (the "Main cloud" ) extends over $\sim$50 pc scale,which is quite different from the other two active star-forming GMCs dominatedby remarkable filaments/shells obtained by our series of studies in M33. Thefraction of the relatively dense gas traced by the $^{13}$CO data with respectto the total molecular mass is only $\sim$2 %, suggesting that their spatialstructure and the density are not well developed to reach an active starformation. The CO velocity analysis shows that the GMC is composed of a singlecomponent as a whole, but we found some local velocity fluctuations in the Maincloud and extra blueshifted components at the outer regions. Comparing the COwith previously published large-scale H I data, we suggest that an externalatomic gas flow supplied a sufficient amount of material to grow the GMC up to$\sim$10$^6$ $M_{\odot}$.

ALMA Observations of Giant Molecular Clouds in M33 III: Spatially Resolved Features of the Star-Formation Inactive Million-solar-mass Cloud