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A large fraction of stars forming in our galaxy are born within clustersembedded in giant molecular clouds. In these environments, the background UVradiation fields impinging upon circumstellar disks can often dominate over theradiation fields produced by each disk's central star. As a result, thisbackground radiation can drive the evaporation of circumstellar disks and leadto the loss of planet forming potential within a cluster. This paper presents adetailed analysis of this process for clusters whose stellar membership fallswithin the range $100 \le N \le 1000$. For these intermediate-sized clusters,the background UV field is often dominated by the most massive stellar member.Due to the steep slope of the initial mass function, the amount of backgroundUV light that bathes clusters of similar size displays significant variance. Asa result, we perform a statistical analysis of this problem by calculatingdistributions of FUV flux values impinging upon star/disk systems for severalcluster scenarios. We find that in the absence of dust attenuation, giantplanet formation would likely be inhibited in approximately half of systemsforming within intermediate-sized clusters regardless of stellar membership. Incontrast, the presence of dust can significantly lower this value, with theeffect considerably more pronounced in more populated clusters.

An Investigation of the Loss of Planet-Forming Potential in Intermediate Sized Young Embedded Star Clusters