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Analyzing the high-resolution CO-line survey of the Galactic plane with theNobeyama 45-m telescope (FUGIN), we show that the star-forming complexG18.15-0.30+51 (G18) at radial velocity of 51 \kms is {a tight tripleassociation of a giant molecular cloud (GMC), HII regions, and a supernovaremnant (SNR).} The kinematical distance of G18 is determined to be $d=3.9\pm0.2$ kpc for near solution for circular rotation, $12\pm 0.2$ kpc for farsolution, or $d=6.1\pm 0.1$, if it is in the 3-kpc expanding ring. The HI-lineabsorption of radio continuum from the HII regions constrains the distance to$5.6 \lesssim d_{\rm SNR}\le 7.6$ kpc. The $\Sigma-D$ (radiobrightness-diameter) relation yields the distance to the SNR of $d_{\rmSNR}=10.1^{+11.5}_{-4.7}$ kpc, allowing for a minimum distance of 5.4 kpc. Fromthese we uniquely determined the distance of G18 to be $6.07\pm 0.13$ kpc inthe 3-kpc expanding ring with the SNR being physically associated. Themolecular mass of the GMC is estimated to be $M_{\rm mol}\sim 3\times 10^5M_\odot$. The ratio of Virial to luminous molecular masses is greater thanunity in the central region and decreases outward to $\lesssim 0.2$ at thecloud edge, indicating that the central region is dynamic, while the entirecloud is stable. We discuss the origin of the G18 triple system and propose asustainable GMC model with continuous star formation.

Giant molecular cloud G18.1-0.3+51 associated with HII regions and supernova remnant in the 3-kpc expanding ring