Cloudy to methodically model the ionised and neutral gas from which these lines originate.]{} [We find that the mid- and far-infrared lines account for $\sim$1% of the total infrared luminosity $\rm{L_{TIR}}$, acting as major coolants of the gas. Haro11 is undergoing a phase of intense star formation, as traced by the brightest line, \[O [iii]{}\] 88 $\mu$m, with $\rm{L_{[O~III]}/L_{TIR}}$ $\sim$ 0.3%, and high ratios of \[Ne [iii]{}\]/\[Ne [ii]{}\] and \[S [iv]{}\]/\[S [iii]{}\]. Due to their different origins, the observed lines require a multi-phase modeling comprising: a compact H [ii]{} region, dense fragmented photodissociation regions (PDRs), a diffuse extended low-ionisation/neutral gas which has a volume filling factor of at least 90%, and porous warm dust in proximity to the stellar source. For a more realistic picture of the ISM of Haro11 we would need to model the clumpy source and gas structures. We combine these 4 model components to explain the emission of 17 spectral lines, investigate the global energy balance of the galaxy through its spectral energy distribution, and establish a phase mass inventory. While the ionic emission lines of Haro11 essentially originate from the dense H [ii]{} region component, a diffuse low-ionisation gas is needed to explain the \[Ne 