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We present the results of the interferometric observations of thecircumstellar disk surrounding MWC 297 in the continuum at 230 GHz (1.3 mm) andin the (J=2-1) rotational transitions of $^{12}$CO,$^{13}$CO and C$^{18}$Ousing the Submillimeter Array. At a distance of 250 pc, MWC 297 is one of theclosest, young massive stars (M$_{\star}$ $\sim$10 M$_{\odot}$) to us. Compactcontinuum emission is detected towards MWC 297 from which we estimate a diskmass (gas+dust) of 0.07 M$_{\odot}$ and a disk radius of $\le$ 80 AU. Ourresult demonstrates that circumstellar disks can survive around massive starswell into their main sequence phase even after they have become opticallyvisible. Complementing our observations with the data compiled from theliterature, we find the submm dust opacity index $\beta$ to be between 0.1 and0.3. If the emission is optically thin, the low value of $\beta$ indicates thepresence of relatively large grains in the disk, possibly because of graingrowth. We do not detect any CO emission associated with the continuum source.We argue that the $^{13}$CO emission from the disk is likely optically thin, inwhich case, we derive an upper limit to the gas mass which implies significantdepletion of molecular gas in the disk. The mass of this disk and theevolutionary trends observed are similar to those found for intermediate massHerbig Ae stars and low mass T Tauri stars.

An evolved disk surrounding the massive main sequence star MWC 297?