In the Magellanic Clouds, a strong UV radiation field coupled with a low metallicity leads to an interstellar medium which is quite different from that of the Galaxy. Since systematic mm-wave or infrared spectroscopic surveys have not been published, most of the chemical and physical consequences remain unknown. We have found a molecular line peak with an exceptionally large column density of dense gas in the LMC. With interstellar nitrogen being highly underabundant and oxygen being only slightly depleted relative to Galactic values, we thus propose to carry out a detailed study of nitrogen and oxygen bearing species (NH3, OH, and H2O) toward this source. The project will be complemented by spectroscopic studies at millimeter wavelengths in order to provide a basic set of molecular data for the dense ISM of the Magellanic Clouds.