In spite of the fact that most stars form in clusters, our understanding of the star formation process is mainly limited to isolated low mass protostars. This is particularly important for massive stars. Since massive stars are formed in clusters, their formation is undoubtedly connected to the fragmentation process of the clumps. However, there is no consensus on how massive and dense cold cores collapse and fragment. We studied G305.136+0.068, a very young and cold (T~15K) forming clump, using ALMA Cycle 1 data, in order to characterize its small-scale structure. This is an ideal target to investigate the initial conditions for high-mass star formation because not only it is cold, but also because it is isolated. Here we present the physical and kinematical characteristics of the clump determined through molecular line and continuum ALMA observations with arcsec resolution.