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We study the incidence of group and filamentary dwarf galaxy accretion intoMilky Way (MW) mass haloes using two types of hydrodynamical simulations:EAGLE, which resolves a large cosmological volume, and the AURIGA suite, whichare very high resolution zoom-in simulations of individual MW-sized haloes. Thepresent-day 11 most massive satellites are predominantly (75%) accreted insingle events, 14% in pairs and 6% in triplets, with higher groupmultiplicities being unlikely. Group accretion becomes more common for faintersatellites, with 60% of the top 50 satellites accreted singly, 12% in pairs,and 28% in richer groups. A group similar in stellar mass to the LargeMagellanic Cloud (LMC) would bring on average 15 members with stellar masslarger than $10^4{~\rm M_\odot}$. Half of the top 11 satellites are accretedalong the two richest filaments. The accretion of dwarf galaxies is highlyanisotropic, taking place preferentially perpendicular to the halo minor axis,and, within this plane, preferentially along the halo major axis. The satelliteentry points tend to be aligned with the present-day central galaxy disc andsatellite plane, but to a lesser extent than with the halo shape. Dwarfsaccreted in groups or along the richest filament have entry points that show aneven larger degree of alignment with the host halo than the full satellitepopulation. We also find that having most satellites accreted as a single groupor along a single filament is unlikely to explain the MW disc of satellites.

The multiplicity and anisotropy of galactic satellite accretion