We present metallicities for the young LMC clusters NGC 1818, 1866 2157, 2136 and 2214. This sample is increased by taking over additional values from literature, so for NGC 1850, 1994, 2004, 2100 from the list of Hodge (1981). The intention is to compare these values with metallicities found in a field population of comparable age. Such a population may be represented by bright Cepheids, for which metallicities based on Washington photometry (Harris 1983) are available. The only young SMC cluster, for which we could estimate a metallicity, is NGC 330. Therefore, a comparison with SMC Cepheids, whose metallicities are also quoted by Harris (1981), can lead to uncertain statements only, until further observations of young SMC clusters will have been made.