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tokens: of destroyed GCs to field populations in the bulges of MW-like galaxies, comparing the predictions with the measurements by Schiavon et al. ( 2017 ). They show that, for most of the MW-like galaxies in their simulated volume, the prediction for f Nr of the metal-poor stellar population is lower than the observations by factors of ∼2–30 (bottom panel of their fig. 4). However, for a few simulated galaxies, the predicted f Nr are in good agreement with the observations. Like the MW, the disc populations of those galaxies are characterized by a bimodal distribution in the α–Fe plane, which is a distinctive feature of the MW disc populations (e.g. Hayden et al. 2015 ; Mackereth et al. 2017 ). Mackereth et al. ( 2018 ) showed that this feature is associated with an atypical accretion history, characterized by intense merging in early times and relative calm since z ∼ 1–1.5. It is noteworthy, however, that Hughes et al. ( 2020 ) predictions for these few MW-like galaxies differ from our measurements with regard to the dependence of f Nr on position in the α–Fe plane. The high frequency of ex-GC stars in the field of simulated galaxies is predominantly due to high-α in situ GC formation and destruction, whereas our data show that the high f Nr in the MW bulge is due to the contribution by the dissolution of low-α accreted GCs. This discrepancy would be alleviated if some of the stars in the accreted region in Fig. 2 were in fact formed in situ (see fig. 2 of Hughes et al. 2020 ), but it is not clear that accounting for such a contamination would completely eliminate the disagreement. 4 SUMMARY The results presented in this paper make use of elemental abundances from APOGEE DR16 along with data from Gaia DR2 to study the chemical and kinematic properties of 146 N-rich stars located within the inner 4 kpc of the Galaxy. Our conclusions can be summarized as follows: We find that there are likely accreted and in situ components to the N-rich population within 4 kpc of the Galactic Centre, identified via chemistry by making a cut in [α/Fe]–[Fe/H] space towards low metallicities (as shown in Fig. 2 ; e.g. Hayes et al. 2018 ; Mackereth et al. 2019 ; Das et al. 2020 ). By making this cut and removing stars without proper motions in Gaia , we select 428 and 13 982 bulge stars that lie in the accreted and in situ positions, respectively, with 25 N-rich stars being located in the accreted and 58 located in the in situ locus. We show that our sample of N-rich stars occupies the same locus as so-called SG GC stars, supporting the idea that they are the by-products of GC destruction/evaporation. We find that there is a significant difference in the kinematic properties of chemically defined accreted and in situ populations. This shows that our chemistry-based distinction of these populations maps into differences in kinematic space. We also find that the accreted bulge field population includes stars that share orbital properties with the GE/S system, although no