We address the issue about the variation of the star cluster frequency ( CF ) in the Large Magellanic Cloud ( LMC ) in terms of the cluster spatial distribution .
We adopted the LMC regions traced by Harris & Zaritsky [ 2009 ] and used an updated version of the cluster database compiled by Baumgardt et al . [ 2013 ] .
The CFs were produced by taking into account an appropriate selection of age bins .
Since the uncertainty in a cluster ’ s age can be large compared to the size of the age bins , we account for the fact that a cluster could actually reside in one of a few adjacent age bins .
We confirm that there exist some variations of the LMC CFs in terms of their spatial distributions , although some caveats should be pointed out .
30 Doradus resulted to be the region with the highest relative frequency of youngest clusters , while the log ( t ) = 9-9.5 ( 1-3 Gyr ) age range is featured by cluster formation at a higher rate in the inner regions than in the outer ones .
We compared the observed CFs to theoretical CFs , which are based on the star formation histories of the field stars in each region of the LMC , and found the former predicting more or fewer clusters than observed depending on the field and age range considered .