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High-energy neutrino and $\gamma$-ray emission has been observed from theGalactic plane, which may come from individual sources and/or diffuse cosmicrays. We evaluate the contribution of these two components through themultimessenger connection between neutrinos and $\gamma$ rays in hadronicinteractions. We derive maximum fluxes of neutrino emission from the Galacticplane using $\gamma$-ray catalogs, including 4FGL, HGPS, 3HWC, and 1LHAASO, andmeasurements of the Galactic diffuse emission by Tibet AS$\gamma$ and LHAASO.We find that the IceCube Galactic neutrino flux is larger than the contributionfrom all resolved sources when excluding promising leptonic sources such aspulsars, pulsar wind nebulae, and TeV halos. Our result indicates that theGalactic neutrino emission is likely dominated by the diffuse emission by thecosmic-ray sea and unresolved hadronic $\gamma$-ray sources. In addition, theIceCube flux is comparable to the sum of the flux of non-pulsar sources and theLHAASO diffuse emission especially above 30 TeV. This implies that the LHAASOdiffuse emission may dominantly originate from hadronic interactions, either asthe truly diffuse emission or unresolved hadronic emitters. Future observationsof neutrino telescopes and air-shower $\gamma$-ray experiments in the Southernhemisphere are needed to accurately disentangle the source and diffuse emissionof the Milky Way.

Decomposing the Origin of TeV-PeV Emission from the Galactic Plane: Implications of Multi-messenger Observations