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abstract: 'Low-metallicity galaxies exhibit different properties of the interstellar medium (ISM) compared to nearby spiral galaxies. Obtaining a resolved inventory of the various gas and dust components of massive star forming regions and diffuse ISM is necessary to understand how those differences are driven. We present a study of the infrared/submillimeter (submm) emission of the massive star forming complex N158-N159-N160 located in the Large Magellanic Cloud. Combining observations from the [[*Spitzer*]{}]{} Space Telescope (3.6-70 [$\mu$m]{}), the [[*Herschel*]{}]{} Space Observatory (100-500 [$\mu$m]{}) and LABOCA (on APEX, 870 [$\mu$m]{}) allows us to work at the best angular resolution available now for an extragalactic source (a few parsecs for the LMC). We observe a remarkably good correlation between the [[*Herschel*]{}]{} SPIRE and LABOCA emission and resolve the low surface brightnesses emission. We use the [[*Spitzer*]{}]{} and [[*Herschel*]{}]{} data to perform a resolved Spectral Energy Distribution (SED) modelling of the complex. Using modified blackbodies, we derive an average “effective" emissivity index of the cold dust component $\beta$$_c$ of 1.47 across the complex. If $\beta$$_c$ is fixed to 1.5, we find an average temperature of $\sim$27K (maximum of $\sim$32K in N160). We also apply the @Galliano2011 SED modelling technique (using amorphous carbon to model carbon dust) to derive maps of the star formation rate, the grain temperature, the mean starlight intensity, the fraction of Polycyclic Aromatic Hydrocarbons (PAH) or the dust mass surface density of the region. We observe that the PAH fraction strongly decreases in the H[ii]{} regions we study. This decrease coincides with peaks in the mean radiation field intensity map. The dust surface densities follow the far-infrared di