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Galactic starburst clusters play a twin role in astrophysics, serving aslaboratories for the study of stellar physics and also delineating thestructure and recent star formation history of the Milky Way. In order toexploit these opportunities we have undertaken a multi-epoch spectroscopicsurvey of the red supergiant dominated young massive clusters thought to bepresent at both near and far ends of the Galactic Bar. Significantspectroscopic variability suggestive of radial pulsations was found for theyellow supergiant VdBH 222 #505. Follow-up photometric investigations revealedmodulation with a period of ~23.325d; both timescale and pulsational profileare consistent with a Cepheid classification. As a consequence #505 may berecognised as one of the longest period Galactic cluster Cepheids identified todate and hence of considerable use in constraining the bright end of theperiod/luminosity relation at solar metallicities. In conjunction with extantphotometry we infer a distance of ~6kpc for VdBH222 and an age of ~20Myr. Thisresults in a moderate reduction in both integrated cluster mass (~2x10^4Msun)and the initial stellar masses of the evolved cluster members (~10Msun). Assuch, VdBH222 becomes an excellent test-bed for studying the properties of someof the lowest mass stars observed to undergo type-II supernovae. Moreover, thedistance is in tension with a location of VdBH 222 at the far end of theGalactic Bar. Instead a birthsite in the near 3kpc arm is suggested; providingcompelling evidence of extensive recent star formation in a region of the innerMilky Way which has hitherto been thought to be devoid of such activity.

A long-period Cepheid variable in the starburst cluster VdBH222