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The bulk of solar flare energy is deposited in the chromosphere. Flare ribbons and footpoints in the chromosphere therefore offer great diagnostic potential of flare energy release and transport processes. High-quality observations from the Interface Region Imaging Spectrograph (IRIS) spacecraft have transformed our view of the Sun's atmospheric response to flares. Since most of the chromospheric lines observed by IRIS are optically thick, forward modelling is required to fully appreciate and extract the information they carry. Reproducing certain aspects of the Mg  ii lines remain frustratingly out of reach in state-of-the-art flare models, which are unable to satisfactorily reproduce the very broad-line profiles. A commonly proposed resolution to this is to assert that very large values of 'microturbulence' is present. We assess the validity of that approach by analysing optically thin lines in the flare chromosphere from the X-class flare SOL2014-10-25T17:08:00, using the derived value of non-thermal width as a constraint to our numerical models. A non-thermal width of the order 10 km s−1 was found within the short-lived red wing components of three spectral lines, with relatively narrow stationary components. Simulations of this flare were produced, and in the post-processing spectral synthesis we include within the downflows a microturbulence of 10 km s−1. While we can reproduce the O  i 1355.598 Å line rather well, and we can capture the general shape and properties of the Mg  ii line, the synthetic lines are still too narrow. [ABSTRACT FROM AUTHOR]