Scaling relations of molecular clouds in the MW wind compared to molecular clouds in the MW disk. In all panels, gray dots indicate the MW disk sample from MD17, the points are the wind clumps studied in this paper from APEX data, color-coded by their parent Hi cloud, while the dark gray triangles are for the MW-C21 cloud from LMT data (Heyer et al. 2025). Full black lines denote the best-fit relations to the disk sample from MD17. Panel (a) σ_v–R relation, best-fit σ_v = 0.48R^0.63; (b) M_mol–R relation, best-fit M_mol = 36.7R^2.2; (c) σ_v–M_mol relation, best-fit ${\sigma }_{\text{v}}=0.19M_{\text{mol}}^{0.27}$ ; (d) M_vir vs. M_mol; (e) α_vir vs. M_mol, best-fit ${\alpha }_{\text{vir}}=2500M_{\text{mol}}^{-0.53}$. In panels (d) and (e), the full red line denotes a virialized cloud (M_mol = M_vir), while the dashed black line indicates the α_vir = 3.3 boundary between gravitationally bound and unbound clouds. The histograms on the y axis of panel (e) show normalized distributions of α_vir marginalized over M_mol for disk clouds (gray) and wind clouds (purple). The extremely large virial parameters, driven by the large velocity dispersions, imply that the clouds are not gravitationally bound.