Scenarios that invoke multiple episodes of star formation within young globular clusters ( GCs ) to explain the observed chemical and photometric anomalies in GCs , require that clusters can retain the stellar ejecta of the stars within them and accrete large amounts of gas from their surroundings .
Hence , it should be possible to find young massive clusters in the local Universe that contain significant amounts ( > 10 % ) of the cluster mass of gas and/or dust within them .
Recent theoretical studies have suggested that clusters in the Large Magellanic Cloud ( LMC ) with masses in excess of 10 ^ { 4 } M _ { \odot } and ages between 30 and \sim 300 Â Myr , should contain such gas reservoirs .
We have searched for H i  gas within 12 LMC ( and 1 SMC ) clusters and also for dust using Spitzer 70 \mu m and 160 \mu m images .
No clusters were found to contain gas and/or dust .
While two of the clusters have H i  at the same ( projected ) position and velocity , the gas does not appear to be centred on the clusters , but rather part of nearby clouds or filaments , suggesting that the gas and cluster are not directly related .
This lack of gas ( < 1 % of the stellar mass ) is in strong tension with model predictions , and may be due to higher stellar feedback than has been previously assumed or due to the assumptions used in the previous calculations .